Evolutionary Synthesis Models of Young Star‐forming Regions: The Influence of Binary Stars

Dionne, Dany; Robert, Carmelle

doi:10.1086/500380

Cited by 21 publications

(17 citation statements)

References 33 publications

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“…For the calculations presented in this work, the mixing layers occur at the outer surface of gas condensations immersed in the radiation field of hot stars permeating supercluster A of NGC 2363. The spectral energy distribution (sed) that we adopted for ϕ * was calculated using the code LavalSB (Dionne & Robert 2006). It corresponds to a newly formed star cluster 1 Myr old, in agreement with the upper age limit derived by Drissen et al (2000).…”

Section: )supporting

confidence: 64%

The broad Hα, [O III] line wings in stellar supercluster A of NGC 2363 and the turbulent mixing layer hypothesis

Binette

Drissen

Úbeda

et al. 2009

A&A

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Context. Supercluster A in the extragalactic H ii region NGC 2363 is remarkable for the hypersonic gas seen as faint extended broad emission lines with a full-width zero intensity of 7000 km s −1 . Aims. We explore the possibility that the observed broad profiles are the result of the interaction of a high-velocity cluster wind with dense photoionized clumps. Methods. The geometry considered is that of near static photoionized condensations at the surface of which turbulent mixing layers arise as a result of the interaction with the hot wind. The approximative treatment of turbulence was carried out using the mixing length approach of Cantó & Raga. The code mappings ic was used to derive the mean quantities describing the flow and to compute the line emissivities within the turbulent layers. The velocity projection in three dimensions of the line sources was carried out analytically. is uncomfortably high and alternative processes that would provide comparable constant acceleration of the emission gas up to 4000 km s −1 might have to be considered.

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Section: )supporting

confidence: 64%

The broad Hα, [O III] line wings in stellar supercluster A of NGC 2363 and the turbulent mixing layer hypothesis

Binette

Drissen

Úbeda

et al. 2009

A&A

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“…SpIOMM large 12 ×12 field of view allows us to study the emission lines over the entire disk, with more than 10 6 spectra using two filters centered on Hβ and Hα, of many nearby galaxies (see also Rousseau-Nepton et al, these proceedings) Cantin (2010) developed an iterative technique to separate the flux from different stellar populations in each OASIS spectrum. In summary : a young population (<15 Myr) is characterized by comparing the equivalent width of Hβ and Hα with starburst models from LavalSB (Dionne & Robert 2006) for an instantaneous burst with a standard initial mass function (i.e. a slope of 2.35 with cutoff masses of 1 and 100 M ).…”

Section: Characteristics Of Stellar Populationsmentioning

confidence: 99%

The Study of Barred Spiral Galaxies with Integral-Field Units

et al. 2010

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Abstract. Integral-Field Units have been used to describe the morphology in numerous continuum and line wavebands of a sample of barred spirals galaxies (some of which known as starbursts and LINERs) and to characterize their gas and stellar populations. The central region of eight galaxies was studied with OASIS and an iterative technique developed to separate superposed stellar populations. Young populations, responsible for nebular emission lines, are found in nuclear structures. Older stellar components are mostly uniformly distributed. The mass distribution of the different populations indicates a long sequence of burst events over the whole galaxy history. An activity of the type composite/transition region is often seen over the whole central region. SpIOMM was also used to map the emission lines over the entire disk of one of these galaxies. Among other results, it confirms the peculiar line ratio.

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“…Prior to their use, the Kurucz (1992) spectra have been fitted using a Legendre function in order to remove their low‐resolution spectral features. The code also includes evolutionary tracks for massive close binary stars, which was not used for the current work since binary stars do not have significant impact on UV line profiles (Dionne 1999; Dionne & Robert 2006).…”

Section: Evolutionary Spectral Synthesis With Lavalsbmentioning

confidence: 99%

Physical properties of young stellar populations in 24 starburst galaxies observed with FUSE*

Pellerin¹,

Robert²

2007

Monthly Notices of the Royal Astronomical Society

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We present the main physical properties of very young stellar populations seen with the Far Ultraviolet Spectroscopic Explorer in 24 individual starbursts. These characteristics have been obtained using the evolutionary spectral synthesis technique in the far‐ultraviolet range with the LavalSB code. For each starburst, quantitative values for age, metallicity, initial mass function slope, stellar mass and internal extinction have been obtained and discussed in details. Limits of the code have been tested. One main conclusion is that most starbursts (and probably all of them) cannot be represented by any continuous star formation burst in the far ultraviolet. Also, quantitative values of various optical diagnostics related to these stellar populations have been predicted. Underlying stellar populations, dominated by B‐type stars, have been detected in NGC 1140, NGC 4449 and possibly NGC 3991. We characterized the young stellar populations of less than 5 Myr in Seyfert 2 nuclei.

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Evolutionary Synthesis Models of Young Star‐forming Regions: The Influence of Binary Stars

Cited by 21 publications

References 33 publications

The broad Hα, [O III] line wings in stellar supercluster A of NGC 2363 and the turbulent mixing layer hypothesis

The broad Hα, [O III] line wings in stellar supercluster A of NGC 2363 and the turbulent mixing layer hypothesis

The Study of Barred Spiral Galaxies with Integral-Field Units

Physical properties of young stellar populations in 24 starburst galaxies observed with FUSE*

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